In mLQC-I, the evolution of the effective (quantum) homogeneous universe is asymmetric with respect to the bounce [1]}, [2]}, [3]}, [4]}. In particular, before the bounce (\(t < t_B\) ), the universe is asymptotically de Sitter,
and only very near the bounce (about several Planck seconds), the Hubble parameter \(H\)  which is negative in the pre-bounce regime suddenly increases to zero at the bounce.
Then, the universe enters a very short super-acceleration phase \(\dot{H} > 0\)  (super-inflation) right after the bounce, which lasts until \(\rho \simeq \rho _c^{\scriptscriptstyle {\mathrm {I}}}/2\) , where \(\dot{H}(t)_{\rho \simeq \frac{1}{2}\rho _c^{\scriptscriptstyle {\mathrm {I}}}} = 0\) .
Afterwards, for a kinetic energy dominated bounce \(\dot{\phi }^2_B \gg V(\phi _B)\) , it takes about \(10^{4} \sim 10^{6}\)  Planck seconds before entering the slow-roll inflation [2]}, [3]}, [4]}.
Introducing the quantity,
\(\lambda _H^2 \equiv \frac{a}{{a^{\prime \prime }} - a\mathfrak {A}_{-}} = - \frac{1}{m_{\text{eff}}},\) 
